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PI type instruments

PI type instruments. Yosuke Minowa Naruhisa Takato , Ikuru Iwata (New Development group, Subaru Telescope). Subaru User’s Meeting 2013 (2014/01/21). PI type instruments. Not necessary to be general purpose instruments, but to be single purpose instruments to pursue PI’s own science.

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PI type instruments

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  1. PI type instruments Yosuke Minowa NaruhisaTakato, Ikuru Iwata (New Development group, Subaru Telescope) Subaru User’s Meeting 2013 (2014/01/21)

  2. PItype instruments • Not necessary to be general purpose instruments, but to be single purpose instruments to pursue PI’s own science. • Can be a test-bed of the latest technology for future instrument development. • Complementary to the facility instruments • Provides opportunities to develop human resources (especially for students) • Smaller scale and shorter turn-around time compared to the facility instruments. • Less supported by Subaru.

  3. PI instrument acceptance procedure • Submit a instrument proposal to the director • Proposal Review based on: • Science merit • Feasibility • Impact on the observatory • Infrastructure • Human resources • Budget • Schedule • If the proposal is accepted, • Subaru will support its installation and provide engineering time. • Science time is not guaranteed (PI team have to apply for the open use time) • The PI team is occasionally requested to report the status to the review committee. • The PI instrument needs to pass several reviews during development and commissioning phases before starting science observations.

  4. Applying open-use time with PI instruments • A fact sheet and performance table must be provided by the PI of the instrument before the deadline of the proposal submission. • Referees of the proposal can assess the feasibility of the proposed science based on these information. • To submit the proposal to the PI instruments, proposers have to obtain the permission from the PI of the instrument and include the instrument group in co-investigators. • Subaru does not support the operation of the PI instruments. • If the proposal is accepted, the members of the PI instrument group have to participate the observations to operate the instruments.

  5. Current lineup of the PI instruments • Cassegrain: • -- fully commissioned • Kyoto-3DII – IPMUPMU? • -- development phase • MIMIZUKU– IoA, Univ of Tokyo • SWIMS– IoA, Univ. of Tokyo • Nasmyth IR: • -- fully commissioned • HiCIAO– NAOJ • -- partly commissioned • Kyoto-3DII – IPMU • SCExAO– Subaru • -- commissioning phase • RAVEN– Univ. of Victoria • --- development phase • GIGMICS-- Nagoya Univ. • CHARIS -- Princeton Univ. • IRD (fiber injection module) -- NAOJ • Coude: • -- development phase • IRD(spectrograph) – NAOJ (Visible, NIR, MIR)

  6. Exoplanet Science instruments • HiCIAO – Coronagraphic Image in Near-Infrared • DI, SDI, PDI with and w/o coronagraph for expoplanet and disk survey • Use with AO188, SCExAO • SEEDS program (120 nights) are on going until S15B • SCExAO – Extreme AO system in Visible and NIR • High-contrast with pupil apodization with PIAA + Coronagraph • Low-order Tip/Tilt IR WFS + High-order visible Pyramid WFS • Speckle nulling, Visible aperture masking interferometry • CHARIS – IFU spectrograph in NIR • Exoplanet search and characterization of its atmosphere • J + H (+ K), R~40, > 1.8” x 1.8” • Use with AO188, SCExAO • IRD – High-Dispersion Spectrograph with laser comb • Systematic radial velocity survey of M-type star • R=70,000, Y, J, H, Optical Frequency Comb (OFC), < 1 m/s • Fiber feed from AO188 (Kasdin’s talk tomorrow for more details)

  7. ExoplanetSceience Instruments:SCExAO Phase I (IR bench) PIAA(pupil apodization) Speckle nulling (labo test) • Phase-I capabilities • Pupil Apodization (PIAA)+Coronagraph • Low-order tip/tilt correction with IR WFS • Quasi-static speckle nulling with DM  SCExAO Phase-I is ready for science PLEASE APPLY IN S14B!

  8. ExoplanetSceience Instruments:SCExAO Phase II (visible bench) Pyramid Wavefront Sensor: Closed loop laboratory performance on 5 Zernike’s at 1.7 kHz. Simulation w/o PWFS w/ PWFS 0 dB frequency = 30 Hz • Pyramid WFS for high-order correction • Provides 90% Strehl Ratio in H-band • Closed loop operation was succeeded in the laboratory. • (1.7kHz with 5Zernike modes, 300Hz with 900 Fourier modes) • On-sky test will be performed on Apr. 2014 • Available for science obs. from S14B or S15A • Competitive to Gemini/GPI or VLT/Sphere • Aperture Masking Interferometry in visible wavelength (guest module) • VAMPIRES (polarization) and FIRST (pupil remapping with fiber) • Small inner working angle (<40mas, better than PIAA+Coronagraph at IR) Correction region

  9. ExoplanetSceience Instruments: IRD • R=70,000 spectral resolution with laser frequency comb generator •  1m/s RV precision • Search for planets in the habitable zone around M dwarfs. • Fiber Injection module will be placed on the movable stage in AO188 optical bench, which enable flexible instrument exchange to IRD from any other AO assisted instruments during the night.  increase the chance of the observation with IRD • First light obs. will be Jan-Mar, 2015. Coude room NsIR Obs. floor

  10. Unique capabilities • Kyoto-3DII: Visible IFU sepctrographand Fabry-Perot imager • Provide the only IFU capability at the Subaru. • Use with AO at NsIR, which provides FWHM~0”.1 at ***-band. • IFU mode was successfully commissioned with AO188 • Fabry-perot mode will be tested during S14A. • CCD will be replaced from EEV to Hamamatsu FDCCD, which largely improve the sensitivity at around 9000A from S14B. • GIGMICS : MIR high-dispersion spectrograph • Study of physical and chemical condition of inter-stellar molecules • Germanium immersion grating echelle spectrograph • Engineering obs. will be conducted somewhere between S14A-15B.  R~40000 at 8-13μm Ge immersion grating

  11. Test Bed • RAVEN --- Multi-Object AO system • Simultaneous observation of two objects within Φ3’.5 FOV • used with IRCS • Test bed for TMT MOAO system • First science demonstrator with MOAO (see Oya-san’s talk for more details) • SWIMS – NIR wide field multi-color imager and MOS muti-color • MIMIZUKU – MIR multi-filed imager and spectrograph • TAO 6.5m telescope’s facility instruments. • Provide opportunities for initial instrument test • Perform early science with Subaru (see Konishi-san and Kamizuka-san’s talk for more details)

  12. Roles of PI instruments in the future • Subaru’s Future Strategy toward 2020 • Strengthen capabilities of wider field survey with HSC, PFS, and GLAO(?). • Most of 1st and 2nd generation facility instruments will be decommissioned. • Important roles of the PI instruments toward 2020 • Accommodate science which does not require wide field (such as exoplanet instruments)  Maintain cutting-edge science capabilities at Subaru • Test bed for TMT’s 2nd generation instruments (such as RAVEN)  Facilitate the TMT’s instrument development  Develop human resources

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